I use the Reimers mass loss rate ([1]}) in the form \(\dot{M}_{\rm wind} \simeq 3 \times 10^{-13} LM^{-1} R M_\odot {~\rm yr}^{-1}\) , where the stellar luminosity \(L\) , mass \(M\) , and radius \(R\)  are in solar units. I note that other expressions are also possible (e.g., [2]}). For this mass loss rate, which is linear with the stellar luminosity, the ratio of the rate at which envelope burning adds helium to the core, \(\dot{M}_{\rm He}\) , to the wind mass loss rate, \(\dot{M}_{\rm wind}\) , is
\(\frac{\dot{M}_{\rm He}}{\dot{M}_{\rm wind}} \simeq 0.3 \left( \frac{M_{\rm rem}}{1.4 M_\odot } \right)\left( \frac{R_{\rm g}}{200 R_\odot } \right)^{-1},\) 
